A New Look at the HS Hydrae System
The result's identifiers
Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F22%3A10455234" target="_blank" >RIV/00216208:11320/22:10455234 - isvavai.cz</a>
Result on the web
<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=S3mvxrhtpw" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=S3mvxrhtpw</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.3847/1538-3881/ac4492" target="_blank" >10.3847/1538-3881/ac4492</a>
Alternative languages
Result language
angličtina
Original language name
A New Look at the HS Hydrae System
Original language description
A growing group of stellar triple systems contains an eclipsing binary for which the depth of eclipses has been proven to change in time, a sign of evolving orbital inclination. The recent analysis of historical observations of HS Hya significantly extended the timespan over which the inclination changes are known for this system. Here we add a few more observations and reanalyze the whole data set with a single methodology. We also improve our own analytical approach to enable describing the secular evolution of the orbital architecture of hierarchical triple systems applicable to the HS Hya case. Analyzing the available photometric and spectroscopic data we obtain two main results. First, the dynamical evolution itself allows to constrain the masses of the stars in the inner binary to 1.31 +/- 0.03 M-circle dot and 1.27 +/- 0.03 M-circle dot, and the mass of the unseen third component to 0.56(-0.09)(+0.12)M(circle dot) (all 95% confidence level results). This makes it an M- or K-type dwarf accompanying the binary. Second, the orbital planes of the inner binary and the third component are significantly noncoplanar, allowing two solutions for their mutual angle J. Either the motion of the third component is prograde, and J is most likely in the 50 degrees -65 degrees range, or the motion is retrograde, and J is most likely in the 120 degrees -150 degrees range. The precession period of both orbital planes about the total angular angular momentum is similar to 700 yr (with about two centuries of uncertainty). This implies HS Hya will become eclipsing again around the year 2200.
Czech name
—
Czech description
—
Classification
Type
J<sub>imp</sub> - Article in a specialist periodical, which is included in the Web of Science database
CEP classification
—
OECD FORD branch
10308 - Astronomy (including astrophysics,space science)
Result continuities
Project
<a href="/en/project/GA21-11058S" target="_blank" >GA21-11058S: Orbital and chemical evolution of emerging planetary systems</a><br>
Continuities
P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)
Others
Publication year
2022
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Data specific for result type
Name of the periodical
The Astronomical Journal
ISSN
0004-6256
e-ISSN
1538-3881
Volume of the periodical
163
Issue of the periodical within the volume
2
Country of publishing house
US - UNITED STATES
Number of pages
14
Pages from-to
94
UT code for WoS article
000750008800001
EID of the result in the Scopus database
2-s2.0-85125477118